The limited angular resolution of our observations (320–800 au) does not allow to probe the disk scale nor the jet launch region. Here, we consider the two following classes of periodic mass-ejection models proposed to account for the wiggling pattern of protostellar outflows: i) jet precession; ii) orbital motion around a binary companion. Both models produce a garden-hose effect [1]}: close to the source the jet propagates almost parallel to the main jet axis while further downstream, the side-to-side wiggling is amplified as the fluid parcels ejected in different directions diverge from each other. Outflow morphology allows discriminating between both models: an anti-symmetric S shape is observed in the precession scenario, while a mirror symmetric W shape is observed in the orbital motion scenario [1]}, [3]}, [4]}, [5]}, [6]}.
